AGN-driven winds and ionized clouds moving along the jet in PKS

Transcription

1 GH 2015: Forming and Fueling Supermassive Black Hole Seeds July 6-24, 2015, Tonantzintla, Puebla AGN-driven winds and ionized clouds moving along the jet in PKS Eric Faustino Jiménez-Andrade V. Chavushyan 1, J. León-Tavares 1, A. Olguín-Iglesias 1, Jari Kotilainen 2 1 INAOE, Mexico 2 University of Turku, Finland

2 Outline Extended emission line regions in radio galaxies PKS , an historical overview Observations (VLT/FORS2, HST/WFC) The central engine (BH mass) Outflow along the jet Summary 7/8/15 Jiménez-Andrade E.F. 2

3 EELR in RG HST (f555w, f702w, f814w) + VLA (25MHz) 3C 266 3C 324 Extended emission line regions (EELR) are often observed around radio galaxies (preferentially at z>0.7). The emission-line profiles of EELR reveal disturbed kinematics and high-velocity motions, ~1000km/s (e.g. Chambers et al. 1990; McCarthy, Baum & Spinrad 1996, Solórzano- Inarrea et al. 2001) These EELR can be up to 100 kpc in size and are often elongated and aligned along the radio jet axis (e.g. Best et al. 1996, Armus et al. 1998). 3C 368 Best et al. (1997) 7/8/15 Jiménez-Andrade E.F. 3

4 EELR in RG Such precise alignments, EELR - radio axes, are contrary to what would be expected for illumination of a central source HST (f555w, f702w, f814w) + VLA (25MHz) The passage of the radio jet through the ISM drives strong shock waves into warm clouds of gas embedded in the hot halo of the galaxy. è the shocked gas is likely to be a strong source of line emission (e.g. Inskip et al. 2002). 7/8/15 Jiménez-Andrade E.F. 4

5 EELR in RG The very large distances of high-redshift radio galaxies make their study difficult. Detailed studies of nearby radio galaxies that share many of the properties of high-redshift radio galaxies have been made (e.g. Tadhunter et al. 1991, Clark et al. 1998, Villa-Martín et al. 1999). In particular, valuable information are derived from long-slit spectra of these low-z objects. 7/8/15 Jiménez-Andrade E.F. 5

6 EELR in RG A jet-induced outflow in 3C293 (z=0.045) WHT With long-slit spectroscopy allows to estimate the spatial extent and kinematics of EELR. In 3C293 a fast outflow of ionized gas was identified (with v~1000 km/s). The outflow is located about 1kpc east of the nucleus, in a region of enhanced radio emission due to the presence of a distorted jet. A rotating ionized gas disc (30 kpc in extent) was identified along the major axis of the host galaxy. WSRT-10MHz + DSS MERLIN + HST(f702w) Emonts et al. (2005) 7/8/15 Jiménez-Andrade E.F. 6

7 EELR in RG A jet-induced outflow in 3C293 (z=0.045) Also, the ionization state can be studied. Density, Temperature Mass of the gas outflow (~10 5 M ) WHT Emonts et al. (2005) 7/8/15 Jiménez-Andrade E.F. 7

8 PKS PKS was classified as a BL Lac (Danziger et al. 1979) (Sbarufatti et al. 2006) (Shaw et al. 2012) (Urry and Padovani, 1995) (Beckmann and Shrader, 2012). 7/8/15 Jiménez-Andrade E.F. 8

9 PKS PKS is among the most remarkable objects in the southern hemisphere. This objects display two striking characteristics: a) This is multi-faceted active galaxy Elliptical host galaxy at z= Danziger et al. (1979) Detected in X-rays by Chandra and in γ-rays by EGRET (Birkinshaw et al. 2002, Lin et al. 1995). Ulrich (1981) On 2010 June 17, a γ-ray flare was detected by the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope (Iafrate et al. 2010). Swift follow-up observation confirmed the high activity of the source in optical, UV, and X-rays (D Ammando et al. 2010). Keel (1986) Scarpa et al. (1995) 7/8/15 Jiménez-Andrade E.F. 9

10 PKS b) It has an optical jet. MAD Ks-band and VLA 15GHz In fact, the morphology of the jet is very similar at radio, near-ir, and optical frequencies. Keel (1986) NTT-SUSI R-band Falomo (1994) Viewing angle: Pian et al º Giroletti et al º - 27 º D Ammando et al º - 12 º Falomo et al. (2009) 7/8/15 Jiménez-Andrade E.F. 10

11 HST image By modeling the host galaxy surface brightness distribution of PKS , we are able to identify an optical jet and and two extended biconical-like structures. GALFIT ( Alejandro Olguín ) The latter structures are located at a distance of 3 kpc. 7/8/15 Jiménez-Andrade E.F. 11

12 Observations We obtained optical spectra with the VLT/FORS2, along the optical jet and the galaxy s optical major axis. VLT-FORS2 HST-f702w VLA-15GHz PA Grism Wavelength range -61 o (jet) GRIS 600B o (major axis) GRIS 600RI /8/15 Jiménez-Andrade E.F. 12

13 Velocity profiles Rotation curve obtained from the Hα 6563 emission line observed in the longslit spectrum taken along the galaxy s optical major-axis. We found tentative evidence of an outflow moving with a maximum projected velocity of -350 km/s (toward us) at 3 kpc from the galaxy nucleus. 7/8/15 Jiménez-Andrade E.F. 13

14 Velocity profiles Velocity profile along the optical jet frame at PA=-61.0 obtained from the [OII,III] 3727, 5007 lines. Linear fit: p-value=0.02, r2=0.26. This function describes a sinusoidal movement of ionized matter along the jet. The farthest detected emission lies at 24 kpc and the velocity reaches a maximum of 100 km/s. 7/8/15 Jiménez-Andrade E.F. 14

15 The central engine We extracted one 1D spectrum from the nuclear region (with an aperture of 1 arcsec ~ 1 kpc) to assure that the information in both spectra are coming from the same region. We applied the Starlight code (Cid-Fernandes et al. 2005) in order to model the observed spectrum and subtract the host galaxy contribution. 7/8/15 Jiménez-Andrade E.F. 15

16 The central engine A multi-gaussian model is fit to the Hβ+[OIII] complex using a χ2 minimization routine to obtain the best-fitting parameters. The Gaussian decomposition indicates that the narrow [O III] 4959,5007 emission lines are composed of more than one Gaussian component è NLR=NLR1+NLR2 (FHWM~1250 km/s and FWHM~400 km/s respectively). Also, the decomposition indicates the existence of a red-shifted broad component (FWHM of 4600 km/s) è inflowing components. 7/8/15 Jiménez-Andrade E.F. 16

17 The central engine We use the relations proposed by (Vestergaard and Peterson, 2006, VP06) to estimate the black hole mass using the Hβ 4862 and 5100 Å continuum luminosities. Moreover, we employ the M BH σ relation proposed by (Gültekin et al. 2009, G09) to estimate the black hole mass from the stellar velocity dispersion. Since the BLR is complex (i.e. highly non- virialized gas) the values for M are merely rough estimates. 7/8/15 Jiménez-Andrade E.F. 17

18 Ionization source along the jet Star formation along the jet? Image of PKS observed in the Ks band (Falomo et al. 2009). 4 kpc 6 kpc 9 kpc 12 kpc In the nuclear region we are observing a QSO like-spectrum. While the spectra taken from knots visible in IR and radio show narrow emission lines. 7/8/15 Jiménez-Andrade E.F. 18

19 Ionization source along the jet In order to segregate between HII region and AGN we are using diagnostic diagrams which involve the [OII] 3727 Å and Hβ 4862 Å relative equivalent widths (Rola, Terlevich & Terlevich, 1997). è RTT diagram. Not a HII region On the other hand, by applying the criteria proposed by Ho, Filippenko & Sargent (1997): Our results? 7/8/15 Jiménez-Andrade E.F. 19

20 Mass of the outflowing gas along the jet If the gas in a line-emitting region is primarily photoionized, the mass can be derived from basic nebular photoionization theory (Osterbrock, 1989). 1 kpc x 10 kpc? n e = 500 cm 3 which leads to a mass of M. Reported values for the density in jet-cloud interaction regions. Derived values are in the range from cm -3, which leads to a mass of 10 5 M M. In previous works of jet-induced outflows: 3C M (Emmonts et al. 2005) NGC x10 4 M (Rosario et al. 2010) 7/8/15 Jiménez-Andrade E.F. 20

21 Summary SMBH mass: M M. Outflowing gas along the major axis extending beyond to 8 kpc. Outflow mass along the jet: >10 4 M. Ionized clouds moving in a helicoidal way along the jet a t d i s t a n c e s b e y o n d t o ~20Kpc! 7/8/15 Jiménez-Andrade E.F. 21

22 Future work We need to secure an optical spectrum covering the range from angstroms to elaborate diagnostic diagrams and identify the ionization source, allowing also to estimate densities to further estimate the mass of the outflow. With IFS observations the physical conditions, gas dynamics and ionization state can be efficiently studied as function of position relative to the nucleus. High-resolution imaging in the CO lines would allow us to determine how much of it is infalling, and what kind of motions are present è ALMA. 7/8/15 Jiménez-Andrade E.F. 22

23 Thanks! 7/8/15 Jiménez-Andrade E.F. 23

24 Somewhere, something incredible is waiting to be known. Carl Sagan Thanks! 7/8/15 Jiménez-Andrade E.F. 24